James Webb Space Telescope (JWST)

The First Light Machine Who is James Webb?

James E Webb was the first administrator of NASA (1961 to 1968)

He supported a program balanced between Science and Human Exploration.

credit: NASA What is FIRST LIGHT?

End of the dark ages: first light and reionization

What are the first luminous objects? What are the first ? How did black holes form and interact with their host galaxies? When did re-ionization of the inter-galactic medium occur? What caused the re-ionization?

… to identify the first luminous sources to form and to determine the ionization history of the early universe.

Hubble Ultra Deep Field A Brief History of Time Planets, Life & Galaxies Intelligence First Galaxies Evolve Form Atoms & Radiation Particle Physics Big Today Bang 3 minutes

300,000 years 100 million years 1 billion COBE years 13.7 Billion years MAP JWST HST Ground Based Observatories First Light

50-to-100 million years after the , the first massive stars started to form from clouds of hydrogen. But, because they were so large, they were unstable and either exploded supernova or collapsed into black holes. These first stars helped ionize the universe and created elements such as He. O-class stars are 25X larger than our sun. ‘First’ stars may have been 1000X larger.

The (modern) Morgan–Keenan spectral classification system, with the temperature range of each class shown above it, in kelvin. The overwhelming majority of stars today are M-class stars, with only 1 known O- or B-class star within 25 . Our Sun is a G- class star. However, in the early Universe, almost all of the stars were O or B-class stars, with an average mass 25 times greater than average stars today.Wikimedia Commons user LucasVB, additions by E. Siegel

Ethan Siegel, FORBES.com, 24 Oct 2018 First Light: Reionization

Neutral ‘fog’ was dissolved by very bright 1st Generation Stars. At 780 M yrs after BB the Universe was up to 50% Neutral. But, by 1 B years after BB is was as we see it today. 787 M yr confirmed by Neutral Hydrogen method.

Redshift Neutral IGM

zz i i .

Lyman Forest Absorption Patchy Absorption Black Gunn-Peterson trough

SPACE.com, 12 October 2011 How do we see first light objects? Redshift

Blue Green Red + + =

5.8 Gyr 2.2 Gyr

3.3 Gyr 1.8 Gyr

2.2 Gyr 1.0 Gyr Redshift The further away an object is, the more its light is redshifted from the visible into the .

To see really far away, we need an infrared telescope. First Galaxy in Hubble Deep Field

At 480 M yrs after big bang (z ~ 10) this one of oldest observed galaxy. Discovered using drop-out technique. (current oldest is 420 M yrs after BB, maybe only 200 M yrs)

Left image is visible light, and the next three in near-infrared filters. The galaxy suddenly pop up in the H filter, at a wavelength of 1.6 microns (a little over twice the wavelength the eye can detect). (Discover, Bad Astronomy, 26 Jan 2011) JWST Summary • Mission Objective – Study origin & evolution of galaxies, stars & planetary systems – Optimized for near infrared wavelength (0.6 –28 m) – 5 year Mission Life (10 year Goal) • Organization – Mission Lead: Goddard Space Flight Center – International collaboration with ESA & CSA – Prime Contractor: Northrop Grumman Space Technology – Instruments: – Near Infrared Camera (NIRCam) – Univ. of Arizona – Near Infrared Spectrometer (NIRSpec) – ESA – Mid-Infrared Instrument (MIRI) – JPL/ESA – Fine Guidance Sensor (FGS) – CSA – Operations: Space Telescope Science Institute Origins Theme’s Fundamental Questions

• How Did We Get Here? • Where Are We Going? • Are We Alone? JWST Science Themes

First Light and Re-Ionization Big Bang

HHPlanetary-30

MStar-16 Formation Galaxy Formation Life

Galaxy Evolution Three Key Facts

There are 3 key facts about JWST that enables it to perform is Science Mission:

It is a Space Telescope

It is an Infrared Telescope

It has a Large Aperture Why go to Space

Atmospheric Transmission drives the need to go to space. Infrared (mid and far/sub-mm) Telescopes (also uv, x-ray, and gamma-ray) cannot see through the Atmosphere

JWST Discovery Space Infrared Light

COLD Why Infrared ? Why do we need Large Apertures? Aperture = Sensitivity

1010 Photographic & electronic detection

Telescopes alone JWST 8

10 HST CCDs

Sensitivity 106 Improvement Photography over the Eye

104 m

102 -

Short’s 21.5” Short’s

eyepiece

Slow f ratios

Huygens

Galileo Rosse’s 72” 100” Wilson Mount 200” Palomar Mount Soviet6 Adapted from Cosmic 48” Herschell’s Discovery, M. Harwit 1600 1700 1800 1900 2000 Sensitivity Matters

GOODS CDFS – 13 orbits HUDF – 400 orbits JWST will be more Sensitive than Hubble or Spitzer

HUBBLE JWST SPITZER

0.8-meter 2.4-meter T ~ 5.5 K T ~ 270 K

6.5-meter 123” x 136” T ~ 40 K λ/D1.6μm~ 0.14” 312” x 312” 324” x 324” λ/D5.6μm~ 2.22” λ/D24μm~ 6.2” JWST 6X more sensitive 132” x 164” 114” x 84” with similar resolution λ/D2μm~ 0.06” λ/D20μm~ 0.64” JWST 44X more sensitive

Wavelength Coverage 1 μm 10 μm 100 μm

HST

JWST

Spitzer How big is JWST?

21st National Space Symposium, Colorado Springs, The Space Foundation How JWST Works

JWST is folded and stowed for launch

Observatory is deployed after launch

JWST Orbits the 2nd Lagrange Point (L2)

239,000 miles (384,000km)

930,000 miles (1.5 million km)

Earth Moon L2 JWST has 4 Science Instruments (0.6 to 28 micrometers) NIRCam: image the first galaxies NIRSpec: simultaneous spectra of 100 galaxies

MIRI: first HD view of infrared universe FGS: sense pointing to 1 millionth degree NIRISS: imagery & spectra of JWST Telescope Requirements

Optical Telescope Element 25 sq meter Collecting Area 2 micrometer Diffraction Limit < 50K (~35K) Operating Temp

Primary Mirror 6.6 meter diameter (tip to tip) < 25 kg/m2 Areal Density < $6 M/m2 Areal Cost 18 Hex Segments in 2 Rings Low (0-5 cycles/aper) 4 nm rms Drop Leaf Wing Deployment CSF (5-35 cycles/aper) 18 nm rms Mid (35-65K Segments cycles/aper) 7 nm rms 1.315 meter Flat to Flat Diameter Micro-roughness <4 nm rms < 20 nm rms Surface Figure Error Fun Fact – Mirror Surface Tolerance

Human Hair Approximate scale Diameter is 100,000 nm (typical)

PMSA Surface Figure Error < 20 nm (rms)

PMSA

JWST Mirror Technology History

) 2 300 240 TRL-6 Testing 2006 2004 NAR 200 JWST Mirror Risk Reduction TRL 6 text text 100 JWST Primary Ball Beryllium Optic Technology Complete Goodrich Mirror vibro-

Areal Density (Kg/m Density Areal Kodak ULE Mirror Selected - TRL 5.5 30 Mirror2002 acoustics 60 Test 15 text 1980 1990 2000 2010 JWST Prime SBMD 2000 Selected JWST Requirement 1998 AMSD Phase 2

AMSD Phase 1 ProcessMirror Material/Technology improvements\ Risk Selection, Reduction September, 2003 * NASA HST, Chandra, SBMD SIRTF Lessons Learned Onset NGST • •ScheduleBeryllium and chosen Tinsley for technicalstaffing identifiedreasons as 1996 SBMDAMSD Phase– 1996 1 – 1999 - TRL 6 by NAR AMSDJWST(cryogenic risksPhase CTE, 2 – thermal2000 conductance, issues with - Implement an active risk SIRTF Monolithic I70 Be Mirror • 0.535 Vendors m diameter selected for management process early in the Manufacturing • glass,Process •stress3 vendorsimprovements issues (Goodrich, with Be via noted) 6 Kodak,-Sigma Study and •studies20 m ROC Sphere program ( Early investiment) followPrime-Ball)on* Contractor identified Schedule potential Selectionand Tinsley schedule staffing savings NMSD • EDU addedidentified• •BerylliumBall as (Beryllium) key as mirror riskJWST mitigation andrisks ITT/Kodak demonstration• (ULE)CryoDown Null deviceproposedselect Figured to(2003) 4 as mirror to options,along 19 nm with rms AMSD Phase 3 •architecturesProcessGoodrichCoating improvementsAdheasion dropped from (coupon AMSD and .5 meter demonstrations)

Based on lessons learned, JWST invested early in mirror technology to address lower areal densities and cryogenic operations Advantages of Beryllium

Very High Specific Stiffness – Modulus/Mass Ratio Saves Mass – Saves Money

High Conductivity & Below 100K, CTE is virtually zero. Thermal Stability Figure Change: 30-55K Operational Range

Beryllium ULE Glass

Y Surface Figure Y X With Alignment X Vertex Y Compensation

X

Gravity

Gravity Vertex

Y Residual with Y X 36 Zernikes X Removed Vertex

15.0 mm

15.015.0 mm mm

Gravity

Vertex Gravity Mirror Manufacturing Process

Blank Fabrication Machining

Machining of Web Structure Completed Mirror Blank

Machining of Optical Surface

Polishing Mirror System Integration Fun Facts – Mirror Manufacturing Before After

Finished Be Billet Mirror Segment

Be dust which is recycled 250 kgs 21 kgs

Over 90% of material is removed to make each mirror segment – want a little mirror with your Be dust? Mirror Processing at Tinsley Tinsley In-Process Metrology Tools

Metrology tools provide feedback at every manufacturing stage:

Rough Grinding CMM Fine Grinding/Rough Polishing Scanning Shack-Hartmann Final Polishing/Figuring/CNF Interferometry PMSA Interferometer Test Stations included: 2 Center of Curvature CGH Optical Test Stations (OTS1 and OTS2) Auto-Collimation Test Station Data was validated by comparing overlap between tools Independent cross check tests were performed at Tinsley and between Tinsley, Ball and XRCF. Leitz CMM CMM was sized to test PMSA Full Aperture Wavefront Sciences Scanning Shack-Hartmann

SSHS provided bridge-data between grind and polish, used until PMSA surface was within capture range of interferometry SSHS provide mid-spatial frequency control: 222 mm to 2 mm Large dynamic range (0 – 4.6 mr surface slope) When not used, convergence rate was degraded. Comparison to CMM (222 - 2 mm spatial periods) 8/1/2006 data

Smooth grind

SSHS CMM 4.7 µm PV, 0.64 µm RMS 4.8 µm PV, 0.65 µm RMS

Point-to-Point Subtraction: SSHS - CMM = 0.27 µm RMS Full Aperture Optical Test Station (OTS) Center of Curvature Null Test measured & controlled: Prescription, Radius & Figure

Results are cross-checked between 2 test stations.

Interferometer Primary Segment Mount CGH

Fold Flat

.M1 AD M .M2

Interferometer .M3CGH Full Aperture Optical Test Station (OTS) Test Reproducibility (OTS-1 Test #1 vs. Test #2) VC6GA294-VC6HA270

Power (Radius Delta: 0.02 mm)

Astigmatism: 4.4 nm RMS

Mid Frequency: 4.3 nm RMS

Total Surface Delta: PV: 373 nm High Frequency: RMS: 7.6 nm 3.9 nm RMS Auto-Collimation Test Auto-Collimation Test provides independent cross-check of CGH Center of Curvature Test Verifies: Radius of Curvature Conic Constant Off-Axis Distance Clocking

Note: is not a full-aperture figure verification test Primary Mirror Segment Assembly at BATC Ball Optical Test Station (BOTS)

Tinsley ambient metrology results are ‘cross-checked’ at BATC BOTS measurements: Measure Configuration 1 to 2 deformation Measure Configuration 2 to 3 deformation Create a Gravity Backout file for use at XRCF Measure Vibration Testing Deformation Measure Vacuum Bakeout Deformation Measure Configuration 2 mirrors for BATC to Tinsley Data Correlation

Interferometer Environmental Enclosure 6 DOF Test Stand and Mirror

CGH Enclosure Door BOTS to Tinsley Initial Comparison

Power

Astigmatism

Mid Frequency

Initially, BOTS and TOTS Radius did not agree. Discrepancy was determined to be caused by High Frequency bulk temperature difference. Agreement is now at 10 nm rms level. PMSA Flight Mirror Testing at MSFC XRCF

Cryogenic Performance Specifications are Certified at XRCF

Gate Valve

He Shrouds

Optical Test Equipment

5DOF Table

Cryo-Vacuum Chamber is 7 m dia x 23 m long JWST Flight Mirror Test Configuration

100” He Shroud

150.27” 15” Chamber 130.14” 90” Lighting

Facility Optical Axis 38.47” 61.69”

Table and Facility Floor Stand-Offs

Table positioning Actuators, 3 places Primary Mirror Cryogenic Tests XRCF Cryo Test

Cryotest #6 Timeline

Cycle 1 Cycle 2 350 Measurement Measurement 300 293K 293K 293K

250

200

150 Temperature Temperature (K)

100

45K 45K 50

25K 0 11-Apr-11 25-Apr-11 9-May-11 23-May-11 6-Jun-11 A5 Date • Survival • Cryo Deployment A4 B6 Temperature • Nominal Measurement • Hexapod Deformation Pose A1 • RoC Actuation Test • Set RoC • Hexapod Envelope Test • Nominal Measurement A2 C3 • Pullout Current & Redundant • Hexapod Tilt Test Test (3 of 6 PMSAs) • Pullout Current & Redundant Test (3 of 6 PMSAs) Mirror Fabrication

Spare Mirrors Flight Mirrors

EDU B8 13.5 nm-rms SM#2 (A type) 5.9 nm-rms 14.9 nm-rms C6 C1 10.4 nm-rms 10.0 nm-rms B7 A1 B2 13.0 nm-rms 15.3 nm-rms 13.1 nm-rms C7 A6 A2 238 nm-rms 18.0 nm-rms 16.5 nm-rms TM 4.3 nm-rms C5 PMS’s C2 14.9 nm-rms 15.4 nm-rms B1 A5 A3 8.0 µm-rms 15.3 nm-rms 9.6 nm-rms B6 A4 B3 FSM 15.2 nm-rms 9.5 nm-rms 8.2 nm-rms 2.3 nm-rms SM#1 C4 C3 33 nm-rms 15.4 nm-rms 14.2 nm-rms B5 8.5 nm - rms SURFACE FIGURE ERROR Total PM Composite: 23.2 nm RMS PM Requirement: 25.0 nm RMS

James Webb Space Telescope: large deployable cryogenic telescope in space. Lightsey, Atkinson, Clampin and Feinberg, Optical Engineering 51(1), 011003 (2012) Gold Coated Mirror Assemblies

EDU Mirrors ≥ 98% at 2 µm

B7

C2 C1

B4 A3 B8B

A6 A5

C6 SM2 C4C

A2 A4

B5 A1 B3

C5 C3

B6 Optical Telescope Assembly Observatory level testing occurs at JSC Chamber A

Verification Test Activities in JSC Chamber-A

Cryo Position Primary Mirror Focus Sweep Test Metrology Stability Test (inward facing sources)

SM

PG PG

AOS

PG PG PM

Crosscheck Tests in JSC Chamber-A

Pupil Alignment Test Rogue Path Test Pass-and-a- Half Test

Primary Mirror End-to-End WFSC WFE Test Demonstration

Chamber A: . 37m tall, 20m diameter, 12m door . LN2 shroud and GHe panels End-to-end optical testing at JSC July 2017 to Nov 2018

5 0 Telescope & instrument module now at Northrop Grumman for integration with the spacecraft bus and sunshield

Space Telescope Transporter for Air Road and Sea (STTARS) 5 1 Integration of Telescope with Spacecraft & Sunshade at Northrop Mobile Cleanroom Moves JWST to Vibe Test at Northrop

Northrop Grumman, 2018 JWST will be transported by ship through Panama Canal to French Guiana for launch during March 2021

Roll on roll off transport ship built in the Netherlands by Merwede Shipyards • Length 116m • Displacement about 4200 metric tons • Garage deck length 95m (plenty of room for STTARS) • Speed: 15 knots

6900 Nautical Miles Approximately 20 days

Space Telescope Transporter for Air Road and Sea (STTARS) JWST Launched on Ariane 5 Heavy

JWST folded and stowed for launch in 5 m dia x 17 m tall fairing French Guiana

Launch from Kourou Launch Center (French Guiana) to L2 JWST vs. HST - orbit

Sun

Earth

Moon HST in Low Earth Orbit, ~500 km up. Imaging affected by proximity to Earth

Second Lagrange Point, 1,000,000 miles away

JWST will operate at the 2nd Lagrange Point (L2) which is 1.5 L2 Million km away from the earth

56 L2 Orbit Enables Passive Cryogenic Operation

Second Lagrange Point (L2) of Sun-Earth System This point follows the Earth around the Sun The orbital period about L2 is ~ 6 months Station keeping thrusters required to maintain orbit Propellant sized for 11 years (delta-v ~ 93

North Ecliptic Pole Continuous 1.6 x 106 km Zˆ Coverage

5° Xˆ 45° Zone North 1.0 x 106 km Yˆ L2

5.0 x 105 km Earth 1.5 x 106 km Toward 360° Lunar Orbit the Sun JWST observes whole sky while remaining

Continuous continuously in shadow of its sunshield Coverage Field of Regard is annulus covering 35% of the sky Zone South Whole sky is covered each year JWST Deployment JWST Science Theme #1

End of the dark ages: first light and reionization

What are the first luminous objects? What are the first galaxies? How did black holes form and interact with their host galaxies? When did re-ionization of the inter-galactic medium occur? What caused the re-ionization?

… to identify the first luminous sources to form and to determine the ionization history of the early universe.

Hubble Ultra Deep Field When and how did reionization occur?

Reionization happened z > 6 or < 1 B yrs after Big Bang. WMAP says maybe twice?

Probably galaxies, maybe quasar

Key Enabling Design Requirements: Deep near-infrared imaging survey (1nJy) Near-IR multi-object spectroscopy Mid-IR photometry and spectroscopy

JWST Observations: Spectra of the most distant quasars Spectra of faint galaxies Studying Early Universe: ‘First’ Galaxies

NASA, ESA, B. Robertson (University of California, Santa Cruz), A. Feild (STScI) https://www.nasa.gov/sites/default/files/thumbnails/image/image2i1607bw.jpg Galaxy GN-z11 is 13.4 B-yrs away, just 400 M-yrs after BB. It is 25X smaller than and has only 1% the mass of Milky Way, but is forming stars 20X faster (produced by large gas inflow). Other ‘first’ galaxies are forming stars 1000X faster. Oldest Star Formation – 250M yrs after BB

Oxygen was detected in the very distant galaxy MACS1149-JD1 using the Atacama Large Millimeter/submillimeter Array (APMA) and ESO's Very Large Telescope (VLT) to determine that star formation started at an unexpectedly early stage, only 250 million years after the Big Bang.

Keith Cowing, SPACEREF.com, 16 May 2018 First Galaxies form in Cosmic Web

Ripples in the early universe formed long filaments of hydrogen gas surrounded by ‘’. Galaxies form at crossing points. Most of universe’s matter is in these filaments and dark matter. This one is 10B light years away.

A filament of the universe’s “cosmic web” is highlighted with parallel curved lines in this image, while a protogalaxy is outlined with an ellipse. The brightest spot (on the lower right side of the ellipse) is the quasar UM287. The other bright spot is a second quasar in the system. The image combines a visible light image with data from the Cosmic Web Imager. CREDIT: Chris Martin/PCWI/Caltech Charles Choi, Space.com, 5 Aug 2015. Hubble Ultra Deep Field – Near Infrared

Near-Infrared image taken with new Wide-Field Camera 3 was acquired over 4 days with a 173,000 second exposure. Hubble Ultra Deep Field – Near Infrared

47 Galaxies have been observed at 600 to 650 Myrs after BB. Hubble Ultra Deep Field – Near Infrared overlaid with Chandra Deep Field South

CREDIT: X-ray: NASA/CXC/U.Hawaii/E.Treister et al; Optical: NASA/STScI/S.Beckwith et al

Keith Cooper, Astronomy Now, 15 June 2011 Taylor Redd, SPACE.com, 15 June 2011

What came first – Galaxies or Black Holes? Each of these ancient 700 M yrs after BB galaxies has a . Only the most energetic x-rays are detected, indicating that the black-holes are inside very young galaxies with lots of gas. First Black Holes

One theory for ‘first’ black holes is direct collapse of ‘first’ stars. Below shows disappearance of 25X times our Sun star without a supernova.

The visible/near-IR photos from Hubble show a massive star, about 25 times the mass of the Sun, that has winked out of existence, with no supernova or other explanation. Direct collapse is the only reasonable candidate explanation.NASA/ESA/C. Kochanek (OSU)

Ethan Siegel, FORBES.com, 24 Oct 2018 WISE is Wide-Field IR ‘finder scope’ for JWST

WISE has found millions of black holes in galaxies previously obscured by dust called hot DOGs, or dust-obscured galaxies.

Nancy Atkinson , Universe Today, on August 29, 2012 Oldest & Brightest Quasar – 770M yrs after BB

This Quasar is 770 million years after Big Bang, is powered by a black hole 2 billion times the mass of our Sun and emits 60 trillion times as much light as the sun. How a black hole became so massive so soon after the Big Bang is unknown.

Image of ULAS J1120+0641, a very “It is like finding a 6-foot-tall child in kindergarten,” distant quasar powered by a black hole with a mass 2 says astrophysicist Marta Volonteri, at the University billion times that of the sun, was created from of Michigan in Ann Arbor. images taken from surveys made by both the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. The quasar The spectra of the light from this (and other early appears as a faint red dot close to the centre. light objects) indicate that the Universe was still CREDIT: filled with significant amounts of neutral ESO/UKIDSS/SDSS hydrogen even 770 Myrs after big bang.

Nadia Drake , Science News, 29 June 2011 Charles Q. Choi, SPACE.com, 29 June 2011 Unexpected “Big Babies”: 800M yrs after BB

Spitzer and Hubble have identified a dozen very old (almost 13 Billion light years away) very massive (up to 10X larger than our Milky Way) galaxies.

At an when the Universe was only ~15% of its present size, and ~7% of its current age.

This is a surprising result unexpected in current galaxy formation models.

Michael Werner, “”, William H. Pickering Lecture, AIAA Space 2007. JWST Science Theme #2:

The assembly of galaxies

How did the heavy elements form? How is the chemical evolution of the universe related to galaxy evolution? What powers emission from galaxy nuclei?

When did the Hubble Sequence form? What role did galaxy collisions play in their evolution? Can we test hierarchical formation and global scaling relations? What is relation between Evolution of Galaxies & Growth/Development of Black Holes in their nuclei? … to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. M81 by Spitzer Formation of Heavy Elements

Carl Sagan said that we are all ‘star dust’. All of the heavy elements which exist in the universe were formed from Hydrogen inside of stars and distributed via supernova explosions. But observations in the visible couldn’t find enough dust. Image of Supernova 1987A, taken in the Dust is cold, therefore, it can only be seen in IR. infrared by Herschel and Spitzer, shows some of the warm dust surrounding it. CREDIT: Pasquale Panuzzo Looking in the IR (with Herschel and Spitzer) at SPACE.com, Taylor Redd, 7 July 2011 Supernova 1987A, 100,000X more dust was seen than in the visible – the total mass of this dust equals about half of our Sun. 2nd Generation Stars – 700M yrs after BB

This star is a 2nd generation star after the big bang because it has trace amounts of heavy elements – meaning that at least one supernova had exploded before it was formed. But its existence contradicts current theories because it has too much Hydrogen and too much and not enough Carbon and other heavy elements.

Nola Taylor Redd, SPACE.com, 31 August 2011; CREDIT: ESO/Digitized Sky Survey 2 Chemical make-up of Early Universe

1.8 B yr after BB gamma-ray burst illuminates neighboring galaxies yielding spectra of their chemical makeup.

Metals in the early universe are higher than expected – indicating that star formation in the early universe was much higher than current theory.

GRB 090323 was first detected on 23 March 2009 by NASA's Fermi space telescope and then the Swift satellite, shortly followed by the ground-based GROND system (Gamma-Ray burst Optical and Near- infrared Detector) at the MPG/ESO 2.2-metre telescope in Chile, as well as ESO's Very Large Telescope (VLT). The VLT observations revealed that the gamma-ray burst injected light through its host galaxy and another nearby galaxy, which are both seen at a redshift of 3.57, equivalent to 12 billion years ago.

DR EMILY BALDWIN, ASTRONOMY NOW, 02 November 2011 Subaru Deep Field: Ancient Supernova 3.7B yrs after BB 22 of 150 ancient supernovae in 10% of Subaru Deep Field 12 occurred around 3.7B yrs after big bang. Supernova were 10X more frequent at this time than today. Supernova helped seed early universe with chemical elements.

Clara Moskowitz, SPACE.com, 05 October 2011 The Hubble Sequence

Hubble classified nearby (present-day) galaxies into Spirals and Ellipticals.

The has extended this to the distant past. Where and when did the Hubble Sequence form?

Galaxy assembly is a process of hierarchical merging Components of galaxies have variety of ages & compositions JWST Observations: Wide-area near-infrared imaging survey Low and medium resolution spectra of 1000s of galaxies at high redshift Targeted observations of galactic nuclei Distant Galaxies are “Train Wrecks” Merging Galaxies = Merging Black Holes Combined Chandra & Hubble data shows two black holes (one 30M & one 1M solar mass) orbiting each other – separated by 490 light-years. At 160 million light-years, these are the closest super massive black holes to Earth. Theory says when galaxies collide there should be major disruption and new star formation. This galaxy has regular spiral shape and the core is mostly old stars. These two galaxies merged with minor perturbations.

Galaxy NGC3393 includes two active black holes X-ray: NASA/CXC/SAO/G.Fabbiano et al; Optical: NASA/STScI Charles Q. Choi, SPACE.com, 31 August 2011 Galaxy Clusters Galaxy clusters are the largest structures in the universe. Bound together by gravity, they require billions of years to form. Galaxy Clusters have been detected as early at 0.6 B-yrs after big bang. Hubble NIR Image of CL J1449+0856, the most distant mature cluster of At 2.6 B-yrs old, this is not the oldest galaxies found. Color added from ESO’s VLT and NAOJ’s Subaru Telescope. observed . But, spectra CREDIT: NASA, ESA, R. Gobat (SPACE.com 09 March 2011 ) indicates that stars in its constituent galaxies are 1 B-yrs old. Thus, may have started forming about 1.5 B-yrs after BB. X-ray data (similar to image) shows glow from cloud of very hot gas that holds cluster together. Most of the mass of the JKCS 041 at 3.7 B-yr after BB may be one of the Universe's oldest clusters. In cluster is in the gas. Chandra image, X-ray emission is shown in blue. Image: NASA/CXC/INAF/S.Andreon (Astronomy Now, 10 May 2010) Galaxy Formation Rings of interstellar dust circulating around Andromeda’s galactic core viewed in Far-IR by the Herschel space observatory.

The brighter the ring, the more active the star fomation. Further out rings are extremely cold, only a few tens of degrees warmer than absolute zero.

Discovery News; Jan 29, 2013 03:00 PM ET // by Ian O'Neill JWST Science Theme #3:

Birth of stars and protoplanetary systems

How do molecular clouds collapse? How does environment affect star-formation? What is the mass distribution of low-mass stars? What do debris disks reveal about the evolution of terrestrial planets?

… to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars, to the genesis of planetary systems.

David Hardy Birth of Stars and Proto-planetary Systems

Deeply embedded protostar Circumstellar disk

Agglomeration & planetesimals Mature planetary system How does environment affect star-formation?

Massive stars produce wind & radiation Either disrupt star formation, or causes it.

Boundary between smallest brown dwarf stars & planets is unknown Different processes? Or continuum?

JWST Observations: Survey dark clouds, “elephant trunks” or “pillars of creation” star-forming regions

TheThe Eagle Eagle Nebula asas seen seen in by the HST infrared How do proto-stellar clouds collapse?

Stars form in small regions collapsing gravitationally within larger molecular clouds.

Infrared sees through thick, dusty clouds

Proto-stars begin to shine within the clouds, revealing temperature and density structure.

Key JWST Enabling Requirements: Barnard 68 in visibleinfrared light High angular resolution near- & mid-IR imagery High angular resolution imaging spectroscopy Spitzer has Found “The Mountains Of Creation”

Michael Werner, “Spitzer Space Telescope”, William H. Pickering Lecture, AIAA Space 2007.

L. Allen, CfA [GTO] The Mountains Tell Their Tale Interstellar erosion & star formation propagate through the cloud

Young (Solar Mass) Stars are Really Young Stars are Shown in Shown in This Panel This Panel

Michael Werner, “Spitzer Space Telescope”, William H. Pickering Lecture, AIAA Space 2007. Stellar Shockwave

Shockwave created by Zeta Ophiuchi which is moving towards the left at about 24 kilometres per second.

STARSTUFF IMAGE by Stuart Gary, ABC Science, 20 July 2015 Star Formation in Dust/Gas Cloud

Herschel discovered 700 newly-forming stars condensing along filaments of dust in a never before penetrated dark cloud at the heart of Eagle Nebula. Two areas glowing brightest in icy blue light are regions where large newborn stars are causing hydrogen gas to shine.

SPACE.com 16 December 2009 Cosmic Breeding Ground for Young Stars

Photos via ESA/Herschel/PACS, SPIRE/Hi-GAL Project. Acknowledgement: UNIMAP / L. Piazzo, La Sapienza – Università di Roma; E. Schisano / G. Li Causi, IAPS/INAF, Italy Composite image of molecular cloud RCW106 using Herschel. Cloud itself consists of (color coded) gases: hydrogen, oxygen, carbon. Young stars are creating pockets in the cloud. Blue is hot.

Cassie Kelly, Dope Space Pics, February 27, 2017 Impossible Stars

100 to 150 solar mass stars should not exist but they do. When a star gets to 8 to 10 solar mass its wind blows away all gas and dust, creating a bubble and stopping its growth (see Herschel Image). Image of RCW 120 (ESA), The bubble shock wave is creating a dense Discover.com, Ian O’Neill, 7 May 2010 2000 solar mass region in which an ‘impossible’ star is forming. It is already 10 solar mass and in a few 100 thousand years will be a massive 100 to 150 solar mass – making it one of the biggest and brightest in the galaxy.

(Space.com, 6 May 2010) Orion Nebula Protoplanetary Discs

Hubble has discovered 42 protoplanetary discs in the Orion Nebula

Credit: NASA/ESA and L. Ricci (ESO) All of Life’s Ingredients Found in Orion Nebula

Herschel Telescope has measured spectra for all the ingredients for life as we know them in the Orion Nebula. (Methanol is a particularly important molecule)

Wired.com Mar 2010 JWST Science Theme #4:

Planetary systems and the origins of life

How do planets form? How are circumstellar disks like our Solar System? How are habitable zones established?

… to determine the physical and chemical properties of planetary systems including our own, and to investigate the potential for the origins of life in those systems. Robert Hurt Planetary Formation Questions and 2 Models Ultima Thule

New Horizons’ imaging of Ultima Thule on 1 Jan 2019 appears to support the Model of Planetary System Formation. History of Known (current) NEO Population

200618001900195019901999 The Inner Solar System in 2006 Known • 340,000 minor planets • ~4500 NEOs Earth • ~850 Crossing Potentially Hazardous Outside Objects (PHOs) Earth’s Orbit

Scott Manley Armagh Observatory Landis, “Piloted Flight to a Near-Earth Object”, AIAA Conference 19 Sep 07 Follow the DUST

Dust disks are durable and omnipresent

The central star of the Helix Nebula, a hot, luminous , shows an infrared excess attributable to a disk in a planetary system which survived the star’s chaotic evolution

Michael Werner, “Spitzer Space Telescope”, William H. Pickering Lecture, AIAA Space 2007. Protoplanetary Disks are Ubiquitous & Diverse

Planets form in the gaps and spiral arms.

Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 Spiral Arms Hint At The Presence Of Planets

Disk of gas and dust around a sun-like star has spiral-arm-like structures. These features may provide clues to the presence of embedded but as-yet-unseen planets.

Near Infrared image from Subaru Telescope shows disk surrounding SAO 206462, a star located about 456 light- years away in the Lupus. Astronomers estimate that the system is only about 9 million years old. The gas- rich disk spans some 14 billion miles, which is more than twice the size of Pluto's orbit in our own solar system.

Photonics Online 20 Oct 2011 10 Jupiter Mass 20 AU from star

Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 ~ 40 years of Protoplanetary Disk research

Photometric measurement as function of wavelength shows gaps.

Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 Protoplanetary disks are complex and dynamic

Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 Protoplanetary disk observations require multiple wavlengths

JWST

Catherine Espaillat (Boston University), Disks to Planets: Observing Planet Formation in Disks Around Young Stars, AAS 2019 Direct Imaging of Planet Formation

ALMA is mm/sub-mm 15-km baseline array telescope producing a 35 mas resolution image. (10 m telescope at 500 nm has 10 mas) HL Tau is 1 million year old ‘sun- like’ start 450 light-years from Earth in constellation Taurus. Concentric rings separated by gaps suggest planet formation.

HL Tau is hidden in visible light Our Planetary System behind a massive envelope of dust ALMA image of the young star HL Tau and its protoplanetary disk. This best and gas. ALMA wavelength sees image ever of planet formation reveals multiple rings and gaps that herald the presence of emerging planets as they sweep their orbits clear of dust and gas. through dust. Credit: ALMA (NRAO/ESO/NAOJ); C. Brogan, B. Saxton (NRAO/AUI/NSF) Eta Corvi System ALMA measures ‘cold’ Kuiper belt debris. Spitzer measures ‘warm’ asteroid belt debris. JWST will provide higher resolution image of asteroid belt.

MacGregor, Disks in Nearby Planetary Systems with JWST and ALMA, AAS 2019 Techniques to Detect Exoplanets

Direct Imaging

108 Direct Imaging detects planets far from their star

HR 8799 has at least 4 planets 3 planets (‘c’ has Neptune orbit) were first imaged by Hubble in 1998. Image reanalyzed because of a 2007 Keck discovery. 3 outer planets have very long orbits or 100, 200 & 400 years. Multiple detections are required to see this motion.

Denise Chow, SPACE.com; 06 October 2011 HR 8799 Planet (b) HR 8799 is 129 light-years from earth, 1.5X the size of our sun in the constellation Pegasus, and has at least 4 planets. HR 8799 Planet (b) is 7X the mass of Jupiter and has water, methane and carbon monoxide in its atmosphere.

RT.com March 13, 2015 Techniques to Detect Exoplanets

Doppler Spectroscopy or Radial Velocity Method

111 Radial Velocity Method finds planets close to stars

61 Virginis (61 Vir) has 3 planets inside of Venus’s orbit. From their star, the planets have masses of ~5X, 18X & 24X Earth’s mass. They orbit 61 Virginis in 4, 38 & 124 day periods. Also,direct Spitzer observations indicate a ring of dust at twice the distance of Neptune from the star.

Bad Astronomy Orbital schematic credit: Chris Tinney Techniques to Detect Exoplanets

Transit Method

113 Transit Method Finds Planets Kepler (launched in 2009) searched for planets by staring at 165,000 stars looking for dips in their light caused when a planet crosses in front of the star.

Kepler has found over 1000 ‘confirmed’ planets and over 4000 potential planets. Confirmed Exoplanets versus Time

115 Census as of 14 Dec 2017

Total Confirmed Exoplanets = 3567 Total found by Kepler = 2525

https://www.nasa.gov/sites/default/files/thumbnails/image/fig10-exoplanetdisc-dec14.jpg Exoplanet Populations & Discovery Method

https://www.nasa.gov/sites/default/files/thumbnails/image/press-web25_exoplanet_populations.jpg Kepler’s Verified Planets, by Size As of May 10, 2016 Final data release: spring 2017

Courtesy: NASA/ARC

118 Small Planets come in Two Sizes

https://www.nasa.gov/sites/default/files/thumbnails/image/press-web19_small_planets_two_sizes-edit.jpg Nearly All Stars have Planets

Credit: NASA/Kepler/F.Fressin

Our galaxy has 100B stars of which 17B are like ours, so our galaxy could have 17B Earth size planets. But only a few will be in Habitable Zone Also, need a moon.

Nancy Atkinson; Universe Today; January 7, 2013 Habitable Zone Life requires water. Liquid water can only exist in the ‘Goldilocks'’ Zone. The hotter the star, the further away the zone.

'Billions of stars' in the Milky Way may have planets that contain alien life, Ellie Zolfagharifard, Dailymail.com, 18 March 2015 All Stars may have 1 to 3 HZ Planets

Titius-Bode law (used to predict Uranus) states that ratio between the orbital period of the first and second planet is the same as the ratio between the second and the third planet and so on. Thus, if you know how long it takes for some planets to orbit a star, you can calculate how long it takes for others to orbit and can calculate their position in the planetary system. Blue dots show planets measured by Kepler in 151 systems. Red boxes predicted ‘missing’ 228 planets Average of 1 to 3 HZ planets per star.

'Billions of stars' in the Milky Way may have planets that contain alien life, Ellie Zolfagharifard, Dailymail.com, 18 March 2015 Kepler Mission

Kepler-11has a star like ours & Kepler 22b is the first in the 6 mini-Neptune size planets habitable zone.

Five of six Kepler-11 exoplanets (all Kepler-22b is located about 600 light- larger than Earth) orbit their star years away, orbiting a sun-like star. Its is closer than Mercury orbits the sun. 2.4 times that of Earth, and the two One orbits inside Venus. planets have roughly similar temperatures (maybe 22C). Credit: NASA/AP (Pete Spotts, Christian Science Monitor.com, 23 May 2011.) CREDIT: NASA/Ames/JPL-Caltech Spitzer Mission: Epsilon Eridani

Epsilon Eridani is a young planetary system only 10.5 light-years away with a structure similar to ours.

Observed with both Spitzer and SOFIA.

Credit: NASA/JPL-Caltech/R. Hurt (SSC)

Credit: NASA/JPL Samantha Mathewson, Space.com | May 4, 2017 124 Spitzer Mission: Trappist-1

Trappist-1 is M-class star – i.e. much cooler than our G-class star.

Thus, the Trappist habitable zone is much closer to its star.

M-class stars may not be friendly to life because they have higher radiation environment than our G-class star.

Credit: NASA/JPL

125 How Spitzer Observed the Trappist-1 System

Credit: NASA/JPL

126 > 100 Habitable Zone Planet Candidates > 25 smaller than 2 Earth Radii

https://www.nasa.gov/sites/default/files/thumbnails/image/press-web15_kepler_hz_planets_edit.jpg Is There Life Elsewhere in the Galaxy?

Why is a large UVOIR space telescope required Number of FGK stars for which Need to multiply these values by Earth x fB SNR=10, R=70 spectrum of Earth- toto getanswer the thisnumber question? of potentially life-bearing twin could be obtained in <500 ksec planets detected by a space telescope. 1000 Habitable Zones (HZ) of nearby stars subtend Earth = fraction of stars with Earth-mass planets in HZ very small angles (<200 mas) fB = fraction of the Earth-mass planets that have detectable biosignatures Earth-mass planets within these HZ will be very 100 faint (>29 AB mag) If: Earth x fB ~1 then DTel ~ 4m x RequiresEarth highfB-contrast< 1 (10then-10) imagingDTel ~ to 8m see 10 planet.Earth Cannotx fB achieve<< 1 thisthen from D theTel ~ground. 16m

Number of nearby stars capable of hosting potentially habitable planets is not large (e.g., Kepler is finding that Earth maybe 1.5% to 1 non-binary, solar type or later). 2.5% (SPACE.COM, 21 Mar 2011) 2-m 4-m 8-m 16-m Sample size  D3 Green bars show the number of Thus,Planets an with 8-m detectable telescope biosignatures might find may1 to be3 FGK stars that could be observed Earthrare. May twins need and to an search 16-m many telescope systems might to find 3x each in a 5-year mission without findeven 10 a handful.to 20 Earth Sample twins. size  D3 exceeding 20% of total observing time available to community.

Marc Postman, “ATLAST”, Barcelona, 2009; Modified by Stahl, 2011 How are habitable zones established?

Titan Source of Earth’s H20 and organics is not known Comets? Asteroids?

History of clearing the disk of gas and small bodiesTitan Role of giant planets?

JWST Observations: Comets, Kuiper Belt Objects Icy moons in outer solar system Where does the water come from?

Spitzer Spectrum Shows Water Vapor Falling onto Protoplanetary Disk

Michael Werner, “Spitzer Space Telescope”, William H. Pickering Lecture, AIAA Space 2007. Proto-Stars produce Water

In a proto-star 750 light-years away, Herschel detected: Spectra of Atomic Hydrogen and Oxygen are being pulled into the star, and Water vapor being spewed at 200,000 km per hour from the poles.

The water vapor freezes and falls back A Protostar and its Polar Jets NASA/Caltech onto the proto-planetary disk.

Discovery is because Herschel’s Other Herschel Data finds enough infrared sensors can pierce the water in the outer reaches of the young star TW Hydrae (175 light- dense cloud of gas and dust feeding yrs from Earth) to fill Earth's the star’s formation. oceans several thousand times over.

Mike Wall, SPACE.com; Date: 20 October 2011 (National Geographic, Clay Dillow, 16 June 2011) Molecular Oxygen discovered in space

Herschel found molecular oxygen in a dense patch of gas and dust adjacent to star-forming regions in the Orion nebula.

The oxygen maybe water ice that coats tiny dust grains.

SPACE.com, 01 August 2011 Search for Habitable Planets atmosphere

habitability

L. Cook interior surface

Sara Seager (2006) Search for Life

What is life?

What does life do?

Life Metabolizes

Sara Seager (2006)

All Earth life uses chemical energy generated from redox reactions

Life takes advantage of these spontaneous reactions that are kinetically inhibited

Diversity of metabolisms rivals diversity of exoplanets

Lane, Nature May 2006 Sara Seager (2006) Bio Markers

Spectroscopic Indicators of Life

Absorption Lines Water Oxygen & Ozone CO2 Methane “Red” Edge “Blue” Haze How to see an Exoplanet’s Atmosphere

One method is absorption spectroscopy during transits. Another is reflected light spectroscopy

Konopacky, High Contrast Imaging and Adaptive Optics for Nearby Stars and Planetary Systems, AAS 2019 Earth Through Time

Kasting Sci. Am. 2004 See Kaltenegger et al. 2006 Earth from the Moon Seager Beyond JWST SLS enables even larger telescope Concepts:

HabEx LUVOIR OST Far-IR Internal Coronagraph Controls Diffraction to Reveal Exoplanets in “Dark Hole” Starshade (External Occulter) Blocks Starlight, Controls Diffraction prior to entering Telescope

142 Direct Imaging

Giant Space Telescopes will be able to directly image Planetary Systems using either internal coronagraphs or external star shades.

Simulated image for a 12-m telescope, a 100-m star shade, and 1 day exposure. R=100 ATLAST Spectrum of 1 Earth-mass Terrestrial Exoplanet at 10 pc Exposure: 51 ksec on 8-m Reflectance  (Planet Mass)2/3 4.3 ksec on 16-m 5 Earth-mass: 8.5 ksec on 8-m Bkgd: 3 zodi

SNR=10 @ 790 nm

H2O

H2O H2O H2O

H2O O2()

O2(B) O2(A)

H2O

O2(A) Detail:

@ 750 nm

Marc Postman, “ATLAST”, Barcelona, 2009 Detecting Photometric Variability in Exoplanets

Ford et al. 2003: Model of broadband photometric temporal variability of Earth

Earth at 10 pc Earth at 20 pc

4-m 8-m 16-m 4-m 8-m 16-m

Require S/N ~ 20 (5% photometry) to detect ~20% temporal variations in reflectivity.

Need to achieve a single observation at this S/N in < 0.25 day of exposure time in order to sample the variability with at least 4 independent observations per rotation period.

Marc Postman, “ATLAST”, Barcelona, 2009 Detecting Photometric Variability in Exoplanets

Graph shows changes in infrared brightness of 2M1207b as measured by Hubble over the course of a 10-hr observation. Change in brightness suggests presence of clouds that influence amount of infrared radiation observed as the planet rotates.

CREDIT NASA, ESA, Y. Zhou (), and P. Jeffries (STScI)

Anthony Watts / February 18, 2016 JWST – the First Light Machine

With its 6X larger collecting aperture, JWST will see back in time further than Hubble and explore the Universe’s first light. Countdown to Launch

JWST is making excellent technical progress Ariane 5 will be ready for launch in 2021 will be the dominant astronomical facility for a decade undertaking a broad range of scientific investigations 1000s of Scientists and Engineers in USA and around the world are working to make JWST.

JWST Full Scale Model Any Questions?